PCP(BSK25)
Abstract
This table corresponds to the zero temperature unified equation of state (EoS) for cold non-accreting neutron stars in beta equilibrium based on the Brussels-Montreal energy- density functional BSk25 [GCP_2013]. Details on the EoS model can be found in Ref. [PCP_2018] and the routines to construct an analytical fit of the EoS are also available on the Ioffe website. The tidal deformability associated to this EoS model was calculated in Ref. [ PCS_2019]. The outer crust was calculated using the Hartree-Fock-Bogoliubov atomic mass table HFB-25 available on the BRUSLIB data base [ XGJCA_2013], except when experimental values were available, for which we used the 2016 Atomic Mass Evaluation [ WGKH_2016], supplemented by the measurements of copper isotopes from Ref. [ W_2017]. The inner crust was computed using the 4th-order Extended Thomas-Fermi (ETF) method with proton shell and pairing corrections added perturbatively via the Strutinsky integral (SI); the nucleon distributions were parametrized using damped Fermi profiles and the Coulomb energy was calculated within the Wigner-Seitz (WS) approximation. Although the EoS was originally calculated ignoring nuclear pastas, their presence in neutron-star crust was later discussed in Refs. [ PCP_2020, PC_2022] and was shown to be marginal in the Extended Thomas-Fermi plus Strutinski Integral framework [ PC_2022]. The core was assumed to be made up by an admixture of neutrons and protons neutralised by electrons and possibly by muons. ^1S_0 neutron and proton pairing gaps in neutron-star cores were calculated in Ref. [ AC_2021].
| Nparam | = | 1 |
| Particles | = | npemN |
| T min | = | 0.0 |
| T max | = | 0.0 |
| T pts | = | 1 |
| nb min | = | 4.68e-10 |
| nb max | = | 1.50e+00 |
| nb pts | = | 479 |
| Y min | = | 0.0 |
| Y max | = | 0.0 |
| Y pts | = | 1 |
Nuclear Matter Properties
| ns | = | 0.1587 | fm-3 |
| E0 | = | 16.032 | Mev |
| K | = | 236.0 | Mev |
| K' | = | 316.5 | Mev |
| J | = | 29.0 | Mev |
| L | = | 36.9 | Mev |
| Ksym | = | -28.5 | MeV |
Neutron Star Properties
| Mmax | = | 2.22 | Msun |
| MDU,e | = | 1.612 | Msun |
| RMmax | = | 11.05 | km |
| R1.4 | = | 12.37 | km |
References
References to the original work:
- [WGKH_2016] M. Wang, G. Audi, F. G. Kondev, W. J. Huang, S. Naimi, and X. Xu, Chinese Physics C41, 030003 (2017)
- [AC_2021] V. Allard and N. Chamel, Universe 7, 470 (2021)
- [PC_2022] J. M. Pearson and N. Chamel, Phys. Rev. C 105, 015803 (2022)
- [PCP_2020] J. M. Pearson, N. Chamel, and A. Y. Potekhin, Phys. Rev. C 101, 015802 (2020)
- [PCP_2018] J. M. Pearson, N. Chamel, A. Y. Potekhin, A. F. Fantina, C. Ducoin, A. K. Dutta, and S. Goriely, MNRAS 481, 2994 (2018)
- [GCP_2013] S. Goriely, N. Chamel, and J. M. Pearson, Phys. Rev. C 88, 024308 (2013)
- [PCS_2019] L. Perot, N. Chamel, and A. Sourie, Phys. Rev. C 100, 035801 (2019)
- [XGJCA_2013] Y. Xu, S. Goriely, A. Jorissen, G. L. Chen, and M. Arnould, Astronomy & Astrophysics 549, A106 (2013)
- [W_2017] A. Welker, et al, Phys. Rev. Lett. 119, 192502 (2017)
Data sheet
Data
| eos.zip (0.17 MB) |
| eos.zip_checksum.txt |
Single files |
| eos.init |
| eos.nb |
| eos.t |
| eos.yq |
| eos.thermo |
| eos.compo |
| eos.mr |
| eos.micro |